
Understanding the origin of our universe, its physical properties, its composition, etc. are among the primary goals of modern science. According to the standard model of cosmology, the theory of the Big Bang proposed by G. Lemaître [1]},  in the year 1927 Historically speaking, A. Friedmann was the first who came up with the idea that the Universe can be dynamic [2]} after finding the solutions of A. Einstein’s field equations. However, he did not link his findings to any astronomical observations. There were many attempts to obtain the dynamic universe solution from Einstein's equations but none of them suggested that the universe is expanding [3]}. It was K. Lundmark in 1924, who estimated extra-galactic distances and suggested that galaxies are red-shifted [4]}. Then in 1927, G. Lemaître discovered new dynamical solutions to Einstein’s equations and obtained the relationship between linear velocity and distance, which he then linked to astronomical observations. This solution was also independently discovered later by H. P. Robertson [5]}, ,  and A. G. Walker [6]}., has been considered the most reliable framework to date to study the evolution of the universe. Extrapolated back in time the Big Bang model gives us crucial information about its origin. According to this model, our universe is expanding and it was much hotter and much smaller in the beginning. The experimental validation of its expansion came after galaxy red-shift measurements by E. Hubble in 1929 [7]}. His observational evidence along with the cosmic microwave background [8]} and Big Bang nucleosynthesis [9]}, [10]} became the key milestones of modern cosmology. To explore the physical properties and the matter content of our universe, physicists have considered different approaches. One of the approaches is the direct astrophysical and astronomical observation, meaning observation at large length scales using telescopes probing different electromagnetic (EM) wavelengths. The other approach is to reproduce the conditions which existed during the very early stages of the universe in terrestrial laboratories producing hot and dense medium in relativistic heavy-ion collisions [11]}, [12]}.
